The official home page of the 2dF QSO Redshift Survey
(2QZ), an Anglo-Australian collaboration surveying 740 square degrees of high-galactic
lattiude sky. It will contain more than 25 000 z<3
QSOs, making it far the largest QSO survey in existence.
This web site describes the survey objectives, current status and
is the primary site for public access to survey data
products. Currently approximately half of the full data set is
available online for download.

AKARI (formerly ASTRO-F) is an infrared sky survey mission from
Institute of Space and Astronautical Science (ISAS) of the Japan
Aerospace eXploration Agency (JAXA) with the participation of the European
Space Agency (ESA).

WWW access to machine based catalagues produced from Cambridge APM
(Automatic Plate Measuring) Machine scans of UKST, POSS1 and POSS2
plates. The catalogues consist of both blue and red plate
catalogues (i.e. O and E for POSS1 and B and
R for UKST and POSS2). The catalogues are complete for
mod(b)>30 degrees in the Northern Hemisphere and partially complete in
the Southern Celestial Hemisphere.

The Parkes 64-m telescope is commencing an HI Southern Sky
and Zone of Avoidance survey in 1996. The survey will
cover redshifts up to 0.04, and be sensitive to objects
with HI mass between 10^6 and 10^10 solar masses, depending
on distance. This will be the first extensive "blind" survey
of the 21cm extragalactic sky.

Aladin is an interactive sky atlas, developed at CDS (Strasbourg,
France), allowing the user to visualize digitized images of any
part of the sky, to superimpose entries from astronomical catalogs
or personal user data files, and to interactively access related
data and information from the Simbad, NED, and Vizier databases
for all known objects in the field. The set
of sky images consists of the STScI Digital Sky Survey
(DSS-I and DSS-II), as well as an ensemble of higher
resolution images (ESO-R and SERC plates) digitized at the MAMA
facility in Paris.

The All Sky Automated Survey is a project which final
goal is photometric monitoring of approx. 10 million stars brighter
than 14 magnitude all over the sky. The prototype instrument,
located at the Las Campanas Observatory (operated by the Carnegie
Institution of Washington), and the data pipeline were developed by
Dr. Grzegorz Pojmanski of the Warsaw University Observatory. There
is a mirror site in the USA.

AGAPE (Andromeda Galaxy and Amplified Pixels Experiment) is a French
collaboration between CNRS (IN2P3 and INSU) and
CEA (DSM/DAPNIA) laboratories. The project is a search
for microlensing on unresolved stars of the Andromeda M31 galaxy
by MACHOs (baryonic dark matter candidates) of the halo of
the Milky Way as well as of the halo of
M31. [in French].

Archeops is an international collaboration aiming at measuring the Cosmic
Microwave background anisotropies in the (sub)millimetre domain on a large
area of the sky and with high angular resolution. The
first balloon flight occured in July 1999 from Trapani ASI
base. Next flights are planned from Kiruna in Sweden in
December 2000 and January 2001.

The ASTROVIRTEL Project, supported by the European Commission and managed
by the ST-ECF on behalf of ESA and ESO, is
aimed at enhancing the scientific return of the ESO/ST-ECF Archive.
It offers the possibility to European Users to exploit it
as a virtual telescope, retrieving and analysing large quantities of
data with the assistance of the Archive operators and personnel.

The APS Catalog of the POSS I contains millions of
entries for stars and galaxies, and the corresponding Image Database
contains their pixels and more. The data behind the Object
Catalog and Image Database are generated from digitized Palomar Observatory
Sky Survey plates. Object Catalog entries include calibrated magnitudes in
two colors, positions to 0.2 arcseconds, confidence measures on neural
network image classifications, colors, and various other useful parameters.

Big Ear is a Kraus-type radio telescope which covers an
area larger than three football fields. The telescope is famous
for discovering some of the most distant known objects in
the universe, and the longest-running SETI (Search for ExtraTerrestrial Intelligence)
project.

The Catalog of Infrared Observations is a database of over
200,000 published infrared observations of more than 10,000 individual astronomical
sources over the wavelength range from 1 to 1000 microns.
The catalog is available for downloading via ftp.

The 1.2 meter Millimeter-Wave Telescope at the Harvard- Smithsonian Center
for Astrophysics and its twin instrument at CTIO in Chile
have been studying the distribution and properties of molecular clouds
in our Galaxy and its nearest neighbours for over 20
years.

DENIS is a deep complete survey of the astronomical sources
of the Southern Sky in 2 near-infrared bands (J at
1.25 micron & K at 2.16 micron) and one optical
band (I at 0.8 micron) simultaneously, using a one meter
ground-based telescope at La Silla (Chile), with limiting magnitudes 18.5,
16.5 and 14.0, respectively.

DENIS is a deep astronomical survey of the Southern Sky
in two near-infrared bands (J at 1.25 µ and K
at 2.16 µ) and one optical band (I at 0.8
µ) simultaneously, conducted by a European consortium, using a one
meter telescope (ESO, La Silla). The survey started in 1996
and is expected to be completed in 2000. The Centre
de Données Astronomiques de Strasbourg (CDS) is implementing the final
point source databases and is providing access of the processed
and calibrated data to the worldwide community.

We undertook a long term project, DIRECT, to obtain the
direct distances to two important galaxies in the cosmological distance
ladder -- M31 and M33, using detached eclipsing binaries (DEBs)
and Cepheids.

The Deep Extragalactic Evolutionary Probe (DEEP) is a multi-year program
which uses the twin 10-m Keck Telescopes and the Hubble
Space Telescope to conduct a large scale survey of distant,
faint, field galaxies.

The Digitized Sky Survey comprises a set of all-sky photographic
surveys in E, V, J, R, and N bands conducted
with the Palomar and UK Schmidt telescopes. The Catalogs and
Surveys Branch (CASB) is digitizing the photographic plates to support
HST observing programs but also as a service to the
astronomical community. Images of any part of the sky
may be extracted from the DSS, in either FITS or
GIF format.

In this (still experimental) server you may find general informations
as well as the latest publications/preprints from the EROS collaboration.
Our main topic is the search for microlensing amplification of
the luminosities of LMC/SMC stars.

This site offers information about the extensive activities of the
Royal Observatory, Edinburgh, a PPARC establishment responsible for building common-user
IR and sub-mm instrumentation and managing telescope sites and data
archive resources, as well as the UK Schmidt Telescope and
the SuperCOSMOS measuring machine. The ROE site also has links
to, or acts as the home page for:

ELAIS is a European collaborative venture to survey around thirteen
square degrees of the sky using the Infrared Space Observatory.
It is the largest single open time project of the
ISO mission and will produce maps and source lists at
7, 15,90 and 175 microns

FIRST -- Faint Images of the Radio Sky at Twenty-cm
-- is a project designed to produce the radio equivalent
of the Palomar Observatory Sky Survey over 10,000 square degrees
of the North Galactic Cap. Using the NRAO Very Large
Array (VLA) and an automated mapping pipeline, we produce images
with 1.8" pixels, a typical rms of 150 Jy, and
a resolution of 5" . At the 0.75 mJy source
detection threshold, there are ~110 sources per square degree, ~35%
of which have resolved structure on scales from 2-30" .

Hipparcos space astrometry mission: Professionals, amateurs, and educators in astronomer
should be interested in the (updated) Hipparcos astrometry mission www
page, maintained by ESA. The monumental Hipparcos and Tycho star
catalogues, with stellar positions, distances, and proper motions, double star
data, and photometry (including thousands of light curves) was completed
in June 1997. The 17-volume publication (including 6 ASCII CD-ROMs)
can be ordered via the www page; the main catalogues
can also be searched on-line, by object or sky region,
with hyperlinks to the principal annexes. An "Educational Page" offers
some ideas for observational projects for amateurs or for student
projects, with the facility to search for the periods of
variable stars interactively.

The Hubble Deep Field (HDF) is a Director's Discretionary program
on HST in Cycle 5 to image a typical field
at high galactic latitude in four wavelength passbands as deeply
as reasonably possible. In order to optimize observing in the
time available, a field in the northern continuous viewing zone
(CVZ) was selected and images were taken for 10 consecutive
days, or approximately 150 orbits. Shorter 1-orbit images were also
obtained of the fields immediately adjacent to the primary HDF
in order to facilitate spectroscopic follow-up by ground-based telescopes. The
observations were carried out from 18-30 December 1995, and the
data are available to the community for study.

The INTErnational Gamma-Ray Astrophysics Laboratory (INTEGRAL) is a medium size
mission of the European Space Agency dedicated to gamma-ray
astronomy. The INTEGRAL Science Data Center (ISDC) located in Geneva
is the link between the astronomical community at large and
the INTEGRAL spacecraft.

The IRAS Point Source Catalog redshift survey is a survey
of (almost) all of the 15,000 galaxies brighter than 0.6
Jansky at 60 microns, over 83% of the whole sky.
The survey is virtually complete as of Jan 1995, and
results on large-scale structure should appear in the next few
months.

The ISO-HDF project has mapped the Hubble Deep Field at
6.7 and 15 microns, using the ISOCAM camera on the
Infrared Space Observatory (ISO). Data and analysis products are made
available to the community via this WWW page. Please note
that the page is no longer actively maintained.

ISOGAL is a 7 and 15 micron survey of the
inner Galactic disk performed with the Infrared Space Observatory (ISO)
camera, ISOCAM, mostly with 6" pixels. The ISOGAL sources
are systematically cross-identified with the KJI sources of the DENIS
survey.

LAMOST is a meridian reflecting Schmidt telescope. Using active optics
technique to control its reflecting corrector makes it a unique
astronomical instrument in combining large aperture with wide field of
view. The available large focal plane may accommodate up to
4000 fibers, by which the collected light of distant and
faint celestial objects down to 20.5 magnitude is fed into
the spectrographs, promising a very high spectrum acquiring rate of
ten-thousands of spectra per night. The telescope will be located
at the Xinglong Station of National Astronomical Observatories. The projectís
budget is RMB 235 millions yuan, about 28.5 million USD.

The MACHO project is
searching for dark matter in the form of Massive Compact
Halo Objects (MACHOs) using gravitational microlensing. We search for these
events by monitoring over 10 million stars every night in
the LMC and Galactic bulge, using the dedicated 50-inch telescope
at Mt. Stromlo.

MCELS is a survey of two of our nearest neighboring
galaxies, the Large and Small Magellanic Clouds. The survey is
done in the bright emission of Hydrogen (Halpha 6563), Sulfur
([S II] 6724), and Oxygen ([O III] 5007) from the
interstellar gas of these two galaxies to study the properties,
kinematics, and dynamics of the "violent" interstellar medium. Although the
project just started recently, one can already see some samples
of the utility as well as the beauty of emission-line
imaging which will be brought to the astronomical community and
the public in general. The survey is performed with the
University of Michigan's Curtis Schmidt telescope, a 0.6/0.9m Schmidt located
on Cerro Tololo and run by CTIO under a cooperative
agreement with the University of Michigan.

The Medium Deep Survey (MDS) is an international project that
uses the Hubble Space Telescope (HST) in Pure parallel mode
to study the nature of faint galaxies in the deepest
regions of the universe. The released MDS database contains model
fits for about 64000 objects in 185 WFPC2 fields, observed
in most cases using the F814W(I), F606W(V) and for few
in F450W(B) photometric filters. Some fields overlap each other, and
duplicate observations of the same object has not yet been
cross-identified.

The Microlensing Observations in Astrophysics (MOA) Project is a joint
Japanese/New Zealand experiment established in 1995 to carry out astrophysical
observations from New Zealand using `gravitational microlensing' and related techniques.

Images of the Milky Way galaxy in the light of
several spectral lines and continuum bands, spanning the electromagnetic spectrum
from radio to high-energy gamma-ray, are presented. The display is
interactive, allowing zooming and panning of the images, each of
which covers the entire sky within ten degrees of the
Galactic plane. Explanatory text and links to the data sources
and references are included. The Multiwavelength Milky Way site is
an educational service of the Astrophysics Data Facility at NASA
Goddard Space Flight Center.

Deep survey of one square degree in total in K'
(19.5) and J with additional optical imaging in B, V,
R, and I. More than 550 spectra have been taken
and galaxy catalogues are available. See Drory et al. 2001
MNRAS 325, 550 for a detailed description.

The Nearby Field Galaxy Survey (NFGS) aims to construct a
spectrophotometric reference atlas and catalog of the observable properties of
~200 nearby field galaxies. This survey is designed to be
a benchmark for interpreting the spectra and imagery of distant
galaxies. The NFGS web-pages are currently hosted and maintained at
the Arizona State University at www.public.asu.edu/~rjansen/nfgs/.

The OGLE project is a long term microlensing survey with
main target being the search for dark matter in the
Galaxy and possibly also in the Magellanic Clouds. The second
phase of the project is realized on a dedicated 1.3m
Warsaw telescope located in Las Campanas Observatory, Chile. Every night
up to 30 million stars are measured in the Galactic
Bulge, LMC and SMC.

This Web page allows the user to obtain "postage stamp"
FITS images of selected, small fields from the NRAO/VLA Sky
Survey (NVSS). Either 1950 or 2000 positions are supported as
are a number of projective geometries. This survey is being
done with the National Radio Astronomy Observatory's Very Large Array
telescope at a wavelength of 20 cm (1.4 GHz) and
is producing images of the sky north of declination -40
deg with a resolution of 45". Both total intensity and
linear polarization is being imaged. This project began in September
1993 and the main body of observations will be finished
in the Summer of 1996. Results are being made available
as they are produced.

The PLANET collaboration is a worldwide network of astronomers with
access to Dutch, South African, and Australian telescopes. The primary
goal of PLANET is the study of microlensing anomalies (departures
from an achromatic point-source, point-lens light curve) through multi-band, rapidly-sampled
photometry. An ultimate goal is to place constraints on the
number and distribution of planets around other stars.

The Sloan Digital Sky Survey is a project to survey
a 10000 square degree area on the Northern sky over
a 5 year period. A dedicated 2.5m telescope is specially
designed to take wide field (3x3 degree) images using a
5x6 mosaic of 2048x2048 CCD's, in five wavelength bands, operating
in scanning mode. The total raw data will exceed 40
TB. A processed subset, of about 1 TB in size,
will consist of 1 million spectra, positions and image parameters
for over 100 million objects, plus a mini-image centered on
each object in every color. The data will be made
available to the public after the completion of the survey.

The UC Berkeley SETI Program, SERENDIP (Search for Extraterrestrial Radio
Emissions from Nearby Developed Intelligent Populations) is an ongoing scientific
research effort aimed at detecting radio signals from extraterrestrial civilizations.
The project is the world's only " piggyback" SETI system,
operating alongside simultaneously conducted conventional radio astronomy observations. SERENDIP is
currently piggybacking on the 1,000-foot dish at Arecibo Observatory in
Puerto Rico, the largest radio telescope in the world.

The Search for Extraterrestrial Intelligence (SETI) Australia Center supports SETI-related
high school and university science education, SETI research and public
outreach programs from the University of Western Sydney Macarthur. Its
research project, Southern SERENDIP, is an eight million channel spectrum
analyzer piggy-backing onto conventional radio astronomy observations for the next
five years at the Parkes 64 metre radio telescope in
NSW,Australia.

The SETI Institute (the Search for Extraterrestrial Intelligence) serves as
an institutional home for scientific and educational projects relevant to
the nature, distribution, and prevalence of life in the universe.
The mission of the SETI Institute is to explore, understand
and explain the origin, nature and prevalence of life in
the universe. The SETI Institute is a private, nonprofit organization
dedicated to scientific research, education and public outreach. Founded in
1984, the Institute today employs over 100 scientists, educators and
support staff. Research at the Institute is anchored by two
centers, each directed by a renowned scientist who holds an
endowed chair.

SETI@home is a scientific experiment that uses Internet-connected computers in
the Search for Extraterrestrial Intelligence (SETI). You can participate by
running a free program that downloads and analyzes batches of
radio telescope data, for signals which may be transimtted by
intelligent extra terrestrial life.

SWIRE is an approved Legacy Progarm of the SIRTF mission.
SWIRE is a wide-area, high galactic latitude, imaging survey to
trace the evolution of dusty, star-forming galaxies, evolved stellar populations,
and active galactic nuclei as a function of environment from
redshifts, z ~ 3, when the Universe was about 2
billion years old, to the present time. SWIRE will survey
approximately 70 square degrees with the MIPS far-infrared camera and
the with the IRAC mid-infrared camera.

STARE (STellar Astrophysics & Research on Exoplanets) uses precise time-series
photometry to search for extrasolar giant planets transiting their parent
stars. An important byproduct of STARE will be an unusually
complete survey of variable stars within its selected fields-of-view.

The examination of the Sandage two-color photographic survey of the
galactic plane taken in support of the Uhuru X-ray satellite
project (1969-1972) is a continuing project headed by Howard Lanning
(CSC/STScI). Several hundred faint UV sources including many old novae,
white dwarfs, cv's, Be shell stars, etc. have been identified
and presented in the literature and posted on the WWW.
The survey comprises over 100 Palomar (48-in.) Oschin Schmidt plates
extending to a limiting B magnitude of ~20.

SkyView is a facility available over the net which allows
users to retrieve data from public all-sky surveys conveniently. The
user enters the position and size of the region desired,
and the surveys wanted and the data is extracted and
formatted for the user. Documentation available through anonymous ftp.

The Sloan Digital Sky Survey's goal is to probe the
large-scale structure of the universe by systematically mapping in detail
one fourth of the sky. The survey will produce a
catalog of roughly 100 million objects, with redshifts to more
than a million galaxies and quasars.

Stardial delivers images of the night sky nearly in real-time
to the world wide web. It is used primarily for
educational purposes. Its archive consists of images taken at 15
minute (sidereal) intervals since July 1996. The survey covers from
0 to -8 degrees declination to 12th magnitude. Highlights and
possible classroom assignments are described.

The Supernova / Acceleration Probe (SNAP) Mission is expected to
provide an understanding of the mechanism driving the acceleration of
the universe. The satellite observatory is capable of measuring up
to 2,000 distant supernovae each year of the three-year mission
lifetime.

SUMSS is a deep radio survey of the entire sky
south of declination -30 degrees, made using the Molonglo Observatory
Synthesis Telescope, operating at 843MHz and recording right-circular polarization.
SUMSS matches (approximately) the resolution and depth of the NRAO-VLA
Sky Survey (NVSS). The principal data products are mosaics which
cover a 4x4 degree square on the sky. The centres
of the mosaics mirror the NVSS centres in the north.
The resolution is 45" x 45"/sin(dec), and the rms noise
limit varies from 1.3 to 2mJy/beam (lower toward the south
celestial pole). The survey began in March 1997 and
will take eight years to complete. SUMSS is suported by
funding from the Australian Research Council. The primary reference
for a description of the survey is: Bock, D.,
Large, M. and Sadler, E.

Infrared detector technology has made such huge advances in the
past decade that the only existing near-infrared sky survey, which
was carried out at Caltech nearly 25 years ago, no
longer serves as a useful context within which to interpret
observations or select sources for study. The University of Massachusetts
is therefore leading a new project, called the Two Micron
All Sky Survey (2MASS), which will canvas the entire sky
for stars and galaxies as much as 50,000 times fainter
than the stars seen in the last survey.

The initial task of the UKST was to construct a
photographic survey of the entire southern sky. The telescope still
takes some 700 plates a year - about half for
current surveys and the remainder taken at the request of
research astronomers around the world. To date the UKST has
taken over 17,000 plates, the plates are stored in the
Plate Library at the Royal Observatory, Edinburgh (ROE) and represent
a huge source of data for the astronomical community. Some
300 active research programmes make use of UKST plate material.
Many plates are copied in the ROE Photolabs and sold
as Sky Atlases or Teaching Packages. In addition to its
photographic role the UKST also has a multi-object fibre spectroscopy
system known as FLAIR.

The very-low frequency sky survey of discrete sources has been
obtained in the Institute of Radio Astronomy of the Ukrainian
National Academy of Sciences (Kharkov, Ukraine) with the UTR-2 radio
telescope at a number of the lowest frequencies used in
contemporary radio astronomy within the range from 10 to 25
MHz.

The VIRMOS project aims to deliver 2 spectrographs for the
ESO- VLT . VIMOS is a visible imaging spectrograph with
outstanding multiplex capabilities, allowing to take spectra of more than
800 objects simultaneously (10 arcsec slits), or spectroscopy of all
objects in a 1x1 arcmin2 area. NIRMOS is a near-infrared
imaging spectrograph with a multiplex of 180 (10 arcsec slits),
and allows spectroscopy of all objects in a 30x30 arcsec2
area. Together VIMOS and NIRMOS allow to get spectroscopy from
0.37 to 1.8 microns, with unsurpassed efficiency for large surveys.

The VST project is a cooperation between the European Southern
Observatory (ESO) and the Capodimonte Astronomical Observatory (OAC) for the
study, design and construction of a wide field alt-az telescope
of 2.6 m aperture, specialized for high quality astronomical imaging
to be installed and operated on Cerro Paranal, next to
ESO's Very Large Telescope (VLT).

VISTA is the Visible and Infrared Telescope for Astronomy: a
4-m Wide Field Survey telescope for the Southern Hemisphere, being
built at Cerro Paranal, close to ESO VLT, by a
consortium of 18 UK universities.

The Vulcan Camera Project, sponsored by NASA Ames Research Center,
is designed to detect transits of large extrasolar planets using
differential photometry. Vulcan uses a 15cm aperture refactor at
Lick Observatory to image a wide field in which ~6000
stars are monitored for two months, in a search for
the ~1% transit signal expect from a 51 Pegasi-type planet.
Vulcan is a ground-based test-bed for the proposed Kepler
Mission to detect Earth-sized exoplanets.

The Whole Earth Telescope (WET) is a collaboration of astronomers
who observe variable stars (white dwarfs and Delta Scuti stars)
and cataclysmic variables Typically twice a year, we coordinate a
global time-series photometry campaign at ~10 observatories worldwide such that
our target objects are visible from the night side of
the planet 24 hours a day

WFCAM is an IR wide field camera for the UK
Infrared Telescope on Mauna Kea. WFCAM will be operational as
an IR imaging survey instrument in late 2002. The camera
has been designed to maximize survey speed at J, H
and K while retaining excellent image quality.

The Wisconsin H-Alpha Mapper will produce a survey of H-Alpha
emission from the interstellar medium (ISM) over the entire northern
sky. The instrument combines a 24-inch telescope and a high-resolution,
6-inch Fabry-Perot spectrometer to achieve 8-12 km/s velocity resolution in
one-degree beams on the sky. By utilizing CCD technology, we
hope to attain a sensitivity level of 0.01 Rayleighs. This
survey, the first of ionized hydrogen in our galaxy, will
be used to explore the spatial and kinematic structure of
the warm ionized component of the ISM. WHAM is currently
at Pine Bluff Observatory but will move to Kitt Peak, Arizona in the Fall of 1996 for the
survey, which should take about 2 years.